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Sigma Draconis, the Bayer designation for this star, was established in 1603 as part of the Uranometria, a star catalogue produced by German celestial cartographer Johann Bayer. The proper name Alsafi was derived from Arabic Athāfi, erroneously transcribed from the Arabic plural Athāfiyy, by which the nomads designated the tripods of their open-air kitchens. It was the name of an association of this star, τ Dra and υ Dra.[10] According to the catalogue of stars in the Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars, Athāfi or Alsafi were the title for three stars: σ Dra as Alsafi, τ Dra as Athāfi I and υ Dra as Athāfi II.[11]

The star is a main sequence dwarf of spectral type K0 V, which has long served as a K0 V spectral standard star.[21][22][23] Its classification as K0 V defines one of the rare anchor points of the Morgan–Keenan system[24] that have remained unchanged since the original 1943 MKK Atlas. The radius has been directly measured using interferometery with the CHARA Array, which yields a result of 77.8% of the Sun's radius.[7] It has 87% of the Sun's mass, but the luminosity of this star is only 43% that of the Sun.[6][7] The projected rotation rate (v sin i) is relatively low at 1.4 km/s.[8] It is considered a slightly metal-poor star, meaning that it has a lower proportion of isotopes with masses more than helium when compared to the Sun.[25]

The temperature, luminosity and surface activity appear to vary slightly in a manner very similar to the sunspot cycle, although the full length of the cycle has not yet been determined.[26] The total variability is among the lowest of all stars that have been measured by the Hipparcos spacecraft.[25]

As of 2013, no Jupiter-size or larger companion had been detected about the star and there was no indication of excess infrared radiation that would be evidence of circumstellar matter (such as a debris disk).[8][27]

Between 2004 and 2013, extensive radial velocity measurements were gathered on Sigma Draconis using the High Resolution Echelle Spectrometer on the Keck Observatory. The Keck/HIRES data indicated a possible period of about 300 days and a likely alias period of 2800 days. Adding data taken with the Automated Planet Finder at the Lick Observatory strengthened and narrowed the 300-day period while reducing the significance of the 2800-day period. The combined analysis suggests there may be a Uranus-mass planet on a 308-day orbit, though the authors do not yet consider the discovery to be publishable as they have not yet attempted to rule out other, non-planetary explanations for the velocity variations.[28]